Prof.
Ocker Cornelis de Jager
(North-West University, Potchefstroom, South Africa)
10/9/08, 11:30 AM
By solving the Euler equations with magnetization constraints, we can establish the time evolution of composite supernova remnants in the interstellar medium. For given pulsar/SNR parameters and ISM density, we obtain the radial profiles of the pulsar wind nebular field strength (for different sigma parameters) and adiabatic loss rates. Using these constraints we then solve for the time...
Dr
Anita Reimer
(Stanford University)
10/9/08, 11:50 AM
Colliding winds of massive stars in binary systems are candidate sites of non-thermal high-energy photon emission. Long since, coincidences between massive star systems/associations and unidentified gamma-ray sources have been proposed. Only now, with the sensitivity of the Fermi Gamma Ray Observatory and current very-high-energy (VHE) Cherenkov instruments, will it be possible to conclusively...
Fabrice Feinstein
(Université Montpellier 2)
10/9/08, 12:10 PM
Shell-type supernova remnants (SNR) are suspected to be hadronic cosmic-ray
(CR) accelerators within our Galaxy. Several shell-type SNR emit very high
energy gamma rays detected with H.E.S.S., including RX J1713.7-3946,
RX J0852.0-4622, RCW 86 and most recently SN 1006. These observations confirm
that these objects accelerate particles up to at least 100 TeV
Dense molecular clouds...
Dr
Ana Yaiza Rodriguez Marrero
(IEEC-CSIC)
10/9/08, 12:30 PM
We present a theoretical model that explains the high energy phenomenology of the neighborhood of SNR IC 443, as observed with the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescope and the Energetic Gamma-Ray Experiment Telescope (EGRET). We interpret MAGIC J0616+225 as delayed TeV emission of cosmic-rays diffusing from IC 443, what naturally explains the displacement between EGRET...
